1 / 32

Solar magnetic fields 3

Solar magnetic fields 3. Philip Judge, High Altitude Observatory, NCAR. What is it we really want to know? [Different from stellar case] How do we measure what we want to know? …solar spectropolarimetry. Examples of what we really need/want to know?. Which processes control:

cutler
Télécharger la présentation

Solar magnetic fields 3

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Solar magnetic fields 3 Philip Judge, High Altitude Observatory, NCAR What is it we really want to know? [Different from stellar case] How do we measure what we want to know? …solar spectropolarimetry

  2. Examples of what we really need/want to know? • Which processes control: • surface field evolution and • the magnetic solar cycle B at the surface, constraints on magnetic flux and helicity∫A.BdV over a solar cycle …requires measurements ofB(r,t) on longer length and time scales

  3. Examples of what we really need/want to know? • what processes control • surface field evolution and • chromospheric/coronal heating • “ dynamics • flaring We should attempt to measure surface B, magnetic free energy (total - potential) Lorentz force j×B, including current sheets requires measurements ofB(r,t) on small length and time scales (flares) up to and including the base of the corona

  4. coronal magnetic free energy can be derived from measurements of magnetic fields at the base in force-free plasma

  5. Conclusion: We must measure vector B • Magnetograph measurements • give BLOS only • yield potential fields (no free energy) in overlying corona • no curl (currents) or uncurl (vector potential) or helicity

  6. An example: Flare physics (Shibata et al 2007) We can measure plasma now Notice- reconnection site It’s time to try to measure the evolving magnetic field

  7. For vector B we must use spectropolarimetry(most lines are not fully split, field is intermittent)

  8. Polarization modulation in time • This is consequential…. unlike in stars, because of • solar evolution (t ~ v / l), l ~ 100 km, v ~ 0.3 cs • atmospheric seeing • let’s look at a rotating waveplate

  9. Spatial as well as temporal modulationremoval of I-> QUV crosstalk with 2 beams In absence of seeing/jitter, a single beam suffices (Solar B SP)

  10. beam splitter D(t) = ΣM3 M2(t) (MC) XT S = M S S = M-1 D ideal solution for Stokes vector Non-Mueller 4xn matrices, n≥4 Diagonality matters In reality we have noise and crosstalk S = (M+Δ)-1 (D+δ), only statistical properties of Δ,δ are knowable

  11. SPINOR spectropolarimeter

  12. SOLIS VSM

  13. Effects of seeing- bad seeing bad seeing good good+destretched good seeing good seeing, destretched

  14. precise spectropolarimetry is starved of photons! 21

  15. Landi Degl'Innocenti (2012 EWASS meeting): λ = 5000 Å, Δλ = 10 mÅ, T= 5800 K, Δx in arcsec, Δt in seconds, telescope aperture D in meters, T system efficiency: Nphot = 1.2 x 109D2 Δx2 ΔtT Critically sampling R = 1.22 λ/D gives for any aperture D: Nphot = 5 x 106 ΔtT photons/ px Realistically, Δt <10s, T <0.1 so Nphot < 5x 106photons/ px PolarizationsensitivityexceedsNphot-1/2~ 5x 10-4 Target sensitivity for low  (force-free) plasmas: 10-4

  16. Optimalspectropolarimetry • Δx2/R must be 10x larger, e.g. • R=λ/Δλ= 120,000 (24mA @ 500nm, v=c/R = 2.4km/s) • Δx= twice diffraction limit (4x flux) • to give Nphot-1/2~ 5 x 10-5

  17. … different from stellar case • We must modulate at frequencies >> 1 kHz to remove seeing • e.g. ZIMPOL instrument (charge-caching detector 100 kHz) • otherwise limited to sensitivity P/I > 0.01 %

  18. 1st 2nd order in dw/w0=wB/w0

  19. Zeeman line splitting Lites 2000

  20. Zeeman-induced polarization Zeeman parameter ζ: ζ = ωL / ωD, ħωL = μB, ωD= ωline V/c. If ζ << 1: QU ~ ζ2 f” transverseB 180 deg ambiguity V ~ ζf’ longitudinal B

  21. Hanle-modified polarization

  22. diagnosing surface MHD processes

  23. Current density Temperature The “right stuff”: Navarro 2005a,b Inversions of Fe I and Ca II lines in a sunspot, hydrostatic, DST 76cm, SPINOR, sensitivity 1.5x10-4 “bandwidth limited”

  24. Measuring magnetic fields in solarchromiospheric/coronal (low beta) plasma is hard 200-2000G Uitenbroek 2011 Ca II 854 nm 200-2000G 31

  25. Measuring magnetic fields in solarlow beta plasma is hard Casini, Judge, Schad 2012ApJ Si I/ He I 1083 nm region FIRS/DST, noise ~ 3x10-4 Instrument fringeremoval using2D PCA

More Related